Beta Ceti

From Wikipedia, the free encyclopedia
Jump to: navigation, search
β Ceti
Diagram showing star positions and boundaries of the Cetus constellation and its surroundings
Cercle rouge 100%.svg

Location of β Ceti (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Cetus
Right ascension 00h 43m 35.37090s[1]
Declination –17° 59′ 11.7827″[1]
Apparent magnitude (V) 2.02[2]
Characteristics
Spectral type K0 III[3]
U−B color index +0.88[2]
B−V color index +1.01[2]
Variable type Rotationally
Astrometry
Radial velocity (Rv) +12.9[4] km/s
Proper motion (μ) RA: +232.55[1] mas/yr
Dec.: +31.99[1] mas/yr
Parallax (π) 33.86 ± 0.16[1] mas
Distance 96.3 ± 0.5 ly
(29.5 ± 0.1 pc)
Absolute magnitude (MV) –0.13[5]
Details
Mass 2.8[6] M
Radius 16.78 ± 0.25[7] R
Luminosity 139.1 ± 7.0[7] L
Surface gravity (log g) 2.7[8] cgs
Temperature 4,797[8] K
Metallicity [Fe/H] –0.09[8] dex
Rotational velocity (v sin i) 18[9] km/s
Age > 1[10] Gyr
Other designations
Deneb Kaitos, Diphda, Difda al Thani, Rana Secunda, 16 Cet, BD–18 115, GCTP 134.00, Gl 31, HD 4128, HIP 3419, HR 188, SAO 147420.[11]
Database references
SIMBAD data
ARICNS data

Beta Ceti (β Cet, β Ceti) is the brightest star in the constellation Cetus. Although it has the Bayer designation "beta", it is actually brighter than Alpha Ceti. It has the traditional names Deneb Kaitos and Diphda. This orange giant is easy to identify due to its location in an otherwise dark section of the celestial sphere. Based on parallax measurements, it lies at an estimated distance of 96.3 light-years (29.5 parsecs) from Earth.[1]

Properties[edit]

Image of orange giant Beta Ceti from NASA's Chandra X-ray Observatory.

Deneb Kaitos has an apparent visual magnitude of 2.02,[2] making it the brightest star in Cetus. The stellar classification of this star is K0 III,[3] although some sources list a classification of G9.5 III[6] indicating that it lies along the dividing line separating G-type from K-type stars. The luminosity class of 'III' means that it is a giant star that has consumed the hydrogen at its core and evolved away from an A-type main sequence star.[6] After passing through the red giant stage, it underwent the helium flash event and is generating energy through the thermonuclear fusion of helium at its core.[12] Beta Ceti will remain in this mode for over 100 million years.[10]

The effective temperature of the star's outer envelope is about 4,797 K,[8] giving it the characteristic orange hue of a K-type star.[13] In spite of its cooler temperature, Deneb Kaitos is much brighter than the Sun with a bolometric luminosity of about 145 times the luminosity of the Sun,[14] resulting from a radius 18[7] times as large as the Sun and a mass that is 2.8 times the Sun's mass.[6]

This star displays flaring activity that results in random outbursts that increase the luminosity of the star over intervals lasting several days. This is a much longer duration than for comparable solar flare activity on the Sun, which typically last for periods measured in hours.[12] In 2005, a relatively high rate of X-ray emission was detected with the XMM-Newton space observatory.[6] It is emitting about 2,000 times the X-ray luminosity of the Sun, allowing the star to be imaged with the Chandra X-ray Observatory.[10]

Etymology[edit]

The traditional name Deneb Kaitos is Arabic ألذنب ألقيتوس ألجنوب - Al Dhanab al Ḳaiṭos al Janūbīyy for "southern tail of Cetus"; it is also known as Diphda, "frog", from the Arabic الضفدع الثاني aḍ-ḍifdaʿ aṯ-ṯānī "the second frog" ("the first frog" is Fomalhaut).[15]

In Chinese astronomy, Deneb Kaitos is called 土司空, Pinyin: Tǔsīkōng, meaning Master of Constructions, because this star is marking itself and stand alone in Master of Constructions asterism, Legs mansion (see : Chinese constellation).[16] 土司空 (Tǔsīkōng), westernized into Too Sze Kung by R.H. Allen and the meaning is "Superintendent of Earthworks." [17]

In culture[edit]

USS Diphda (AKA-59) was a U.S. Navy ship.

See also[edit]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99), Bibcode:1966CoLPL...4...99J 
  3. ^ a b Montes, D. et al. (November 2001), "Late-type members of young stellar kinematic groups - I. Single stars", Monthly Notices of the Royal Astronomical Society 328 (1): 45–63, arXiv:astro-ph/0106537, Bibcode:2001MNRAS.328...45M, doi:10.1046/j.1365-8711.2001.04781.x 
  4. ^ Wielen, R. et al. (1999), Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions (35), Astronomisches Rechen-Institut Heidelberg, Bibcode:1999VeARI..35....1W 
  5. ^ Elgarøy, Øystein; Engvold, Oddbjørn; Lund, Niels (March 1999), "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity", Astronomy and Astrophysics 343: 222–228, Bibcode:1999A&A...343..222E 
  6. ^ a b c d e Sägesser, S. N.; Jordan, C. (March 2005). Favata, F.; Hussain, G. A. J.; Battrick, B., eds. "Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, held 5-9 July, 2004 in Hamburg, Germany". European Space Agency. p. 931. Bibcode:2005ESASP.560..931S.  |chapter= ignored (help)
  7. ^ a b c Berio, P. et al. (November 2011), "Chromosphere of K giant stars. Geometrical extent and spatial structure detection", Astronomy & Astrophysics 535: A59, arXiv:1109.5476, Bibcode:2011A&A...535A..59B, doi:10.1051/0004-6361/201117479 
  8. ^ a b c d Massarotti, Alessandro et al. (January 2008). "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity". The Astronomical Journal 135 (1): 209–231. Bibcode:2008AJ....135..209M. doi:10.1088/0004-6256/135/1/209. 
  9. ^ "Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 2010-09-30. 
  10. ^ a b c "Beta Ceti: Giant Star's Corona Brightens with Age". Chandra Photo Album. Harvard-Smithsonian Center for Astrophysics. February 20, 2009. Retrieved 2011-12-28. 
  11. ^ "bet Cet -- Variable Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-09-30. 
  12. ^ a b Ayres, Thomas R.; Osten, Rachel A.; Brown, Alexander (November 2001). "3 Ms in the Life of β Ceti: Sustained Flare Activity on a Clump Giant Detected by the Extreme Ultraviolet Explorer". The Astrophysical Journal 562 (1): L83–L86. Bibcode:2001ApJ...562L..83A. doi:10.1086/337971. 
  13. ^ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16 
  14. ^ Kaler, James B. "DENEB KAITOS (Beta Ceti)". University of Illinois. Retrieved 2010-09-30. 
  15. ^ Allen, Richard H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 163. ISBN 0-486-21079-0. Retrieved 2010-12-12. 
  16. ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 9 日
  17. ^ Star Name - R.H. Allen p. 160

External links[edit]